The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

M. Bazot, M. J. Ireland, D. Huber, T. R. Bedding, A. M. Broomhall, T. L. Campante, H. Carfantan, W. J. Chaplin, Y. Elsworth, J. Meléndez, P. Petit, S. Théado, V. Van Grootel, T. Arentoft, M. Asplund, M. Castro, J. Christensen-Dalsgaard, J. D. Do Nascimento, B. Dintrans, X. DumusqueH. Kjeldsen, H. A. McAlister, T. S. Metcalfe, M. J.P.F.G. Monteiro, N. C. Santos, S. Sousa, J. Sturmann, L. Sturmann, T. A. Ten Brummelaar, N. Turner, S. Vauclair

Research output: Contribution to journalArticlepeer-review


The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

Original languageEnglish (US)
Article numberL4
JournalAstronomy and Astrophysics
Issue number1
StatePublished - Dec 13 2010


  • methods: data analysis
  • stars: individual: 18 Sco
  • stars: oscillations
  • techniques: interferometric
  • techniques: radial velocities

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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